Comparing simulated and observed EMIC wave amplitudes using
We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Saikin, A.A. [verfasserIn] Jordanova, V.K. [verfasserIn] Zhang, J.C. [verfasserIn] Smith, C.W. [verfasserIn] Spence, H.E. [verfasserIn] Larsen, B.A. [verfasserIn] Reeves, G.D. [verfasserIn] Torbert, R.B. [verfasserIn] Kletzing, C.A. [verfasserIn] Zhelavskaya, I.S. [verfasserIn] Shprits, Y.Y. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2018 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Journal of atmospheric and solar-terrestrial physics - Amsterdam [u.a.] : Elsevier Science, 1950, 177, Seite 190-201 |
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| Übergeordnetes Werk: |
volume:177 ; pages:190-201 |
| DOI / URN: |
10.1016/j.jastp.2018.01.024 |
|---|
| Katalog-ID: |
ELV000374555 |
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| 245 | 1 | 0 | |a Comparing simulated and observed EMIC wave amplitudes using |
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| 520 | |a We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. | ||
| 650 | 4 | |a EMIC waves | |
| 650 | 4 | |a Van Allen Probes | |
| 650 | 4 | |a Linear theory | |
| 650 | 4 | |a Wave generation | |
| 700 | 1 | |a Jordanova, V.K. |e verfasserin |4 aut | |
| 700 | 1 | |a Zhang, J.C. |e verfasserin |4 aut | |
| 700 | 1 | |a Smith, C.W. |e verfasserin |4 aut | |
| 700 | 1 | |a Spence, H.E. |e verfasserin |4 aut | |
| 700 | 1 | |a Larsen, B.A. |e verfasserin |4 aut | |
| 700 | 1 | |a Reeves, G.D. |e verfasserin |4 aut | |
| 700 | 1 | |a Torbert, R.B. |e verfasserin |4 aut | |
| 700 | 1 | |a Kletzing, C.A. |e verfasserin |4 aut | |
| 700 | 1 | |a Zhelavskaya, I.S. |e verfasserin |4 aut | |
| 700 | 1 | |a Shprits, Y.Y. |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Journal of atmospheric and solar-terrestrial physics |d Amsterdam [u.a.] : Elsevier Science, 1950 |g 177, Seite 190-201 |h Online-Ressource |w (DE-627)320607291 |w (DE-600)2020910-1 |w (DE-576)259485195 |x 1364-6826 |7 nnns |
| 773 | 1 | 8 | |g volume:177 |g pages:190-201 |
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| 936 | b | k | |a 38.81 |j Atmosphäre |
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2018 |
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10.1016/j.jastp.2018.01.024 doi (DE-627)ELV000374555 (ELSEVIER)S1364-6826(17)30212-2 DE-627 ger DE-627 rda eng 530 DE-600 38.81 bkl 39.22 bkl Saikin, A.A. verfasserin aut Comparing simulated and observed EMIC wave amplitudes using 2018 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. EMIC waves Van Allen Probes Linear theory Wave generation Jordanova, V.K. verfasserin aut Zhang, J.C. verfasserin aut Smith, C.W. verfasserin aut Spence, H.E. verfasserin aut Larsen, B.A. verfasserin aut Reeves, G.D. verfasserin aut Torbert, R.B. verfasserin aut Kletzing, C.A. verfasserin aut Zhelavskaya, I.S. verfasserin aut Shprits, Y.Y. verfasserin aut Enthalten in Journal of atmospheric and solar-terrestrial physics Amsterdam [u.a.] : Elsevier Science, 1950 177, Seite 190-201 Online-Ressource (DE-627)320607291 (DE-600)2020910-1 (DE-576)259485195 1364-6826 nnns volume:177 pages:190-201 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GEO SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.81 Atmosphäre 39.22 Astrophysik AR 177 190-201 |
| spelling |
10.1016/j.jastp.2018.01.024 doi (DE-627)ELV000374555 (ELSEVIER)S1364-6826(17)30212-2 DE-627 ger DE-627 rda eng 530 DE-600 38.81 bkl 39.22 bkl Saikin, A.A. verfasserin aut Comparing simulated and observed EMIC wave amplitudes using 2018 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. EMIC waves Van Allen Probes Linear theory Wave generation Jordanova, V.K. verfasserin aut Zhang, J.C. verfasserin aut Smith, C.W. verfasserin aut Spence, H.E. verfasserin aut Larsen, B.A. verfasserin aut Reeves, G.D. verfasserin aut Torbert, R.B. verfasserin aut Kletzing, C.A. verfasserin aut Zhelavskaya, I.S. verfasserin aut Shprits, Y.Y. verfasserin aut Enthalten in Journal of atmospheric and solar-terrestrial physics Amsterdam [u.a.] : Elsevier Science, 1950 177, Seite 190-201 Online-Ressource (DE-627)320607291 (DE-600)2020910-1 (DE-576)259485195 1364-6826 nnns volume:177 pages:190-201 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GEO SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.81 Atmosphäre 39.22 Astrophysik AR 177 190-201 |
| allfields_unstemmed |
10.1016/j.jastp.2018.01.024 doi (DE-627)ELV000374555 (ELSEVIER)S1364-6826(17)30212-2 DE-627 ger DE-627 rda eng 530 DE-600 38.81 bkl 39.22 bkl Saikin, A.A. verfasserin aut Comparing simulated and observed EMIC wave amplitudes using 2018 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. EMIC waves Van Allen Probes Linear theory Wave generation Jordanova, V.K. verfasserin aut Zhang, J.C. verfasserin aut Smith, C.W. verfasserin aut Spence, H.E. verfasserin aut Larsen, B.A. verfasserin aut Reeves, G.D. verfasserin aut Torbert, R.B. verfasserin aut Kletzing, C.A. verfasserin aut Zhelavskaya, I.S. verfasserin aut Shprits, Y.Y. verfasserin aut Enthalten in Journal of atmospheric and solar-terrestrial physics Amsterdam [u.a.] : Elsevier Science, 1950 177, Seite 190-201 Online-Ressource (DE-627)320607291 (DE-600)2020910-1 (DE-576)259485195 1364-6826 nnns volume:177 pages:190-201 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GEO SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.81 Atmosphäre 39.22 Astrophysik AR 177 190-201 |
| allfieldsGer |
10.1016/j.jastp.2018.01.024 doi (DE-627)ELV000374555 (ELSEVIER)S1364-6826(17)30212-2 DE-627 ger DE-627 rda eng 530 DE-600 38.81 bkl 39.22 bkl Saikin, A.A. verfasserin aut Comparing simulated and observed EMIC wave amplitudes using 2018 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. EMIC waves Van Allen Probes Linear theory Wave generation Jordanova, V.K. verfasserin aut Zhang, J.C. verfasserin aut Smith, C.W. verfasserin aut Spence, H.E. verfasserin aut Larsen, B.A. verfasserin aut Reeves, G.D. verfasserin aut Torbert, R.B. verfasserin aut Kletzing, C.A. verfasserin aut Zhelavskaya, I.S. verfasserin aut Shprits, Y.Y. verfasserin aut Enthalten in Journal of atmospheric and solar-terrestrial physics Amsterdam [u.a.] : Elsevier Science, 1950 177, Seite 190-201 Online-Ressource (DE-627)320607291 (DE-600)2020910-1 (DE-576)259485195 1364-6826 nnns volume:177 pages:190-201 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GEO SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.81 Atmosphäre 39.22 Astrophysik AR 177 190-201 |
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10.1016/j.jastp.2018.01.024 doi (DE-627)ELV000374555 (ELSEVIER)S1364-6826(17)30212-2 DE-627 ger DE-627 rda eng 530 DE-600 38.81 bkl 39.22 bkl Saikin, A.A. verfasserin aut Comparing simulated and observed EMIC wave amplitudes using 2018 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. EMIC waves Van Allen Probes Linear theory Wave generation Jordanova, V.K. verfasserin aut Zhang, J.C. verfasserin aut Smith, C.W. verfasserin aut Spence, H.E. verfasserin aut Larsen, B.A. verfasserin aut Reeves, G.D. verfasserin aut Torbert, R.B. verfasserin aut Kletzing, C.A. verfasserin aut Zhelavskaya, I.S. verfasserin aut Shprits, Y.Y. verfasserin aut Enthalten in Journal of atmospheric and solar-terrestrial physics Amsterdam [u.a.] : Elsevier Science, 1950 177, Seite 190-201 Online-Ressource (DE-627)320607291 (DE-600)2020910-1 (DE-576)259485195 1364-6826 nnns volume:177 pages:190-201 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GEO SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.81 Atmosphäre 39.22 Astrophysik AR 177 190-201 |
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Enthalten in Journal of atmospheric and solar-terrestrial physics 177, Seite 190-201 volume:177 pages:190-201 |
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Enthalten in Journal of atmospheric and solar-terrestrial physics 177, Seite 190-201 volume:177 pages:190-201 |
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Atmosphäre Astrophysik |
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EMIC waves Van Allen Probes Linear theory Wave generation |
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Journal of atmospheric and solar-terrestrial physics |
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Saikin, A.A. @@aut@@ Jordanova, V.K. @@aut@@ Zhang, J.C. @@aut@@ Smith, C.W. @@aut@@ Spence, H.E. @@aut@@ Larsen, B.A. @@aut@@ Reeves, G.D. @@aut@@ Torbert, R.B. @@aut@@ Kletzing, C.A. @@aut@@ Zhelavskaya, I.S. @@aut@@ Shprits, Y.Y. @@aut@@ |
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2018-01-01T00:00:00Z |
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Saikin, A.A. |
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Saikin, A.A. ddc 530 bkl 38.81 bkl 39.22 misc EMIC waves misc Van Allen Probes misc Linear theory misc Wave generation Comparing simulated and observed EMIC wave amplitudes using |
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530 DE-600 38.81 bkl 39.22 bkl Comparing simulated and observed EMIC wave amplitudes using EMIC waves Van Allen Probes Linear theory Wave generation |
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ddc 530 bkl 38.81 bkl 39.22 misc EMIC waves misc Van Allen Probes misc Linear theory misc Wave generation |
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ddc 530 bkl 38.81 bkl 39.22 misc EMIC waves misc Van Allen Probes misc Linear theory misc Wave generation |
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Elektronische Aufsätze Aufsätze Elektronische Ressource |
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Journal of atmospheric and solar-terrestrial physics |
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Comparing simulated and observed EMIC wave amplitudes using |
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Comparing simulated and observed EMIC wave amplitudes using |
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Saikin, A.A. |
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Journal of atmospheric and solar-terrestrial physics |
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Journal of atmospheric and solar-terrestrial physics |
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Saikin, A.A. Jordanova, V.K. Zhang, J.C. Smith, C.W. Spence, H.E. Larsen, B.A. Reeves, G.D. Torbert, R.B. Kletzing, C.A. Zhelavskaya, I.S. Shprits, Y.Y. |
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Elektronische Aufsätze |
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Saikin, A.A. |
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10.1016/j.jastp.2018.01.024 |
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530 |
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verfasserin |
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comparing simulated and observed emic wave amplitudes using |
| title_auth |
Comparing simulated and observed EMIC wave amplitudes using |
| abstract |
We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. |
| abstractGer |
We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. |
| abstract_unstemmed |
We perform a statistical study calculating electromagnetic ion cyclotron (EMIC) wave amplitudes based off in situ plasma measurements taken by the Van Allen Probes’ (1.1–5.8 Re) Helium, Oxygen, Proton, Electron (HOPE) instrument. Calculated wave amplitudes are compared to EMIC waves observed by the Electric and Magnetic Field Instrument Suite and Integrated Science on board the Van Allen Probes during the same period. The survey covers a 22-month period (1 November 2012 to 31 August 2014), a full Van Allen Probe magnetic local time (MLT) precession. The linear theory proxy was used to identify EMIC wave events with plasma conditions favorable for EMIC wave excitation. Two hundred and thirty-two EMIC wave events (103 H+-band and 129 He+-band) were selected for this comparison. Nearly all events selected are observed beyond L = 4. Results show that calculated wave amplitudes exclusively using the in situ HOPE measurements produce amplitudes too low compared to the observed EMIC wave amplitudes. Hot proton anisotropy (A hp ) distributions are asymmetric in MLT within the inner (L < 7) magnetosphere with peak (minimum) A hp , ∼0.81 to 1.00 (∼0.62), observed in the dawn (dusk), 0000 < MLT ≤ 1200 (1200 < MLT ≤ 2400), sectors. Measurements of A hp are found to decrease in the presence of EMIC wave activity. A hp amplification factors are determined and vary with respect to EMIC wave-band and MLT. He+-band events generally require double (quadruple) the measured A hp for the dawn (dusk) sector to reproduce the observed EMIC wave amplitudes. |
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| title_short |
Comparing simulated and observed EMIC wave amplitudes using |
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Jordanova, V.K. Zhang, J.C. Smith, C.W. Spence, H.E. Larsen, B.A. Reeves, G.D. Torbert, R.B. Kletzing, C.A. Zhelavskaya, I.S. Shprits, Y.Y. |
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